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DDance
Beyond COVID-19 with. . .Joshua Taylor
Across Hamilton, Canada and the world, artists have been forced to react and adapt to the postponement or cancellation of shows and the closing of venues. Many artists and organizations are rising to meet the complex challenges of COVID-19 even as the pandemic creates waves of news or information that can feel frightening or confusing. Through online platforms, new communities and connections are being forged and art is continuing to be shared with fellow creators and enthusiastic, and grateful audiences.
Beyond Covid-19 brings together writers from Beyond James with members of the Hamilton Arts Community to discuss broad, arts-related topics through digital conversations. A timer is set, and no answers are sought- rather, it's an exchange of ideas and dialogues, which is then presented and shared through Beyond James.
In this edition of Beyond Covid-19, Beyond James' Rebekka Gondosch sat down with Defining Movement Dance's Josh Taylor to discuss how his personal artistic practice, and organization, have evolved as a result of Covid-19. Please note that this conversation has been edited for length.
Rebekka: I'd like to begin by asking you, first off, how you're doing, how you're coping in this wild time, what's been making your heart really happy? How's that been going?
Josh: […] I've been able to do dance classes, I've been able to see my students. I really felt for all my dancers and everyone everywhere who's had, who's been like, working towards a goal only to be like…you can no longer do it. […] I was saying this to a friend the other day, it's like being on a basketball team, going to practice, and never being able to play a game and your season's over. It's just practice, right. And there's so many things to get from practice and like that build up, there's so much skill building and…as dancers and performers like you live for that performance, to be able to perform, to be able to battle, to be able to compete. So I feel for them. But it's been really nice to be able to see my students, at least their faces, and for them to see each other and that's been really joyous to see how they interact at any given time at some classes I'll, I kinda step back for a few minutes and just let them go and talk and chat and make jokes and put on filters and, you know. So, I'm doing alright but uh…it's like up and down but for the most part I feel pretty up. I feel fortunate.
Rebekka: I have so much to already ask. Can this be five hours long?
Josh: Yeah yeah!
Rebekka: I think it's so interesting that you're doing Zoom classes for some reason because the online presence I've seen of you has been through Instagram or I've taken Lisa [Emmon]'s class on YouTube, I didn't even think of the interaction of a Zoom class. Of course that would also be happening, which is fantastic.
Josh: […] part of it was because when this first happened, so around like the 15th or 14th or something, and they made that announcement, and I was already kinda following it, and everything was pointing to we might be shut down for a couple weeks. I was like, okay. A couple of weeks is fine. However, I've got a bunch of dancers who have competition in three weeks so I've gotta make sure I keep them moving. You know, because I don't want them to fall behind and we had some really difficult competitions so I'm like, you know what, let's just get everything online and work to make it happen within the week; so right by the end of March break we're already going online with a version of our full class schedule in terms of DMD. So like you know, about four or five hours of classes per night. So that was like the motivation and I was thinking, I'm like, ahhh these guys are gonna get bored.
And me, I'm gonna get bored. So like, I'm gonna want a little bit of class so that was my original motivation thinking it would be a few weeks and, you know, doing some reading at the beginning while I was setting that up I, you know, the more I was seeing I'm like oh, this is not going to be two weeks this is going to be a long time. And […] just you know in terms of talking with my staff I'm like, you know, let's shift our mindset from this is a few weeks and it's like how can you really work with this new medium of this is your class, and this is what you're doing with your, you know, your competitive group like, what do you do with that. So yeah it uh… zoom has been my every evening for, you know, for about four hours, four/five hours almost yeah, so.
Rebekka: I can empathize with that.
Josh: Zooooom!
Rebekka: Zoom…our best friend.
Josh: Yeah!
Rebekka: Our worst enemy.
Josh: Yeah! Cause there's some days it's great and I'm like, ah this is amazing! And all of a sudden I'm like, wait I can't, I'm sorry guys, just wait there's something happening in the…I'm just gonna try to share the music. Oh no it's cutting out. And then like especially with young children they're like, Josh you're cutting out! Josh there's–
The first few classes was like, you know, I'm not gonna say the word on here but it was a dumpster fire almost.
Rebekka: Bless. Bless the Zoom.
Josh: Yeah, bless it!
Rebekka: A So you moved quite quickly, from what I'm hearing, to online, kinda realized that some things were working, some weren't. How do you feel like things have evolved or shifted? Has the spirit and energy of DMD has it changed, has the community changed? The connection?
Josh: Oh absolutely. […] It's changed and I feel the loss; I think a lot of our community, families, and the dancers, I think we're all feeling that loss and actually what I was sending an email out about, you know, not having our recital, our in-person recital, which is such a celebration of, you know, all the different aspects of the full year of dancers coming together to celebrate on stage and we do like…you know…yeah we do this big recital and the responses coming from that email were you know, how they missed the community, they miss seeing everybody, they miss being in the studio.
There's this energy when you're coming into class and another class is ending and there's this chatter that happens in between and people are saying hi and you know hugging and hi five and then you go into class and that class goes, even when classes don't start right on time there is this energy that is so…you can feel it, you can touch it, you know? And it's like it actually makes each class have this real fire every single time because of the passing through and the different dancers cause it's not always the same groups it might be a competitive group, or the rec, or older or young and…there's that. The little kids seeing the older dancers who they are inspired by every week and the…you know we have a big tech class where dancers who are 17 and 18 and dancers who are 7, you know, and seeing them battle face to face and encourage each other and that and then of course there's all our adult classes and that energy and being able to feed off of what your students are giving you. So I think like it has changed and…you know and that's tough, that's really tough, because it really does give so much energy to everybody who's there. Even when you're exhausted because you've been dancing for hours, you know? But I mean, with that said, we're/it's still connected which is great but you can definitely feel the energy is different and, you know with some of those students who were working towards a goal it did feel, I think for some of them, that the carpet had been taken right underneath them. Some who were in their last year and will not be able to compete with their team again and…I get the feeling that they, especially lately, it's the first two weeks you're like, Oh we don't know what's going to happen but then it starts to sink in that like, there's no competitions, there's no…there's no competing, you're not graduating, you're not getting the recitals, you're not getting these things; so I think for them you can see, I can see their energy…feel kind of heavy? In class, you know? Because you're reminded, it's like you're seeing everybody, or you're seeing what you love and you're doing what you love but you're also, at the same time, reminded what you're not getting. Of being in the walls and, you know, being able to bump people you know, and…yeah. […] So it's changed, but it's still there.
Rebekka: What wisdom or advice or energy do you pass on to students like that? Students who don't know what's coming next, the students who have to grieve the loss of not being able to compete, or their graduation so to speak…
Josh: Um…it's tricky cause I mean we're all in it together right? […] what I've told them, I think one of the turning points I did see in our classes was, okay everyone, this is not ending. At least for a while. And I think where the disappointment was coming from, that heaviness, part of it was the… the idea of…when are things going to open? When are we gonna get back to it? When are we back? And hoping for that and then, you know, take a moment to be like, you know, this is what it is right now. So rather than think about what, you know, thinking about how and when we're going to get back because we don't know and that's going to make you even more anxious and worry more because you're going to want to like, am I going to be able to do this? Am I going to miss this? It's like, you have to accept it and then change […] look at what you have, work with what you have and um…so I have with some of those students, I've talked about the idea of, hey make some dances, make some stuff, now's the time as a artist and as a, you know, a growing artist…put some work, make some work; your instagram page can be your mini resume, it can be your CV for, especially when it comes to dancing and the way the industry it works now with so many of the videos and TikTocks and all of that online…that is like take advantage and like learn some classes, put that stuff online. And don't stop learning and then the other thing is kinda remind them, you know, you didn't get into dancing to compete, you didn't get into dancing because…or very specifically that, you know um, you got into it because of how it makes you feel and although you can't physically connect with people, we are at a time where you can make something, put it up, and people can connect with you that way so, take advantage of that if you can because that's where we are. We're not in the other place, you know and…that was the best I could do. I wish I had a maybe a more inspiring one.
Rebekka: I don't know Josh, that sounds profound to me! That sounds pretty profound.
Josh: Well, I think it sunk in with some of them and some of them I've seen you know, made videos and put some stuff online and got wonderful feedback and I think that's really fun for them. Yeah and I hope, I hope they continue that, I hope dancers continue that and, and I've also said to them, and at the same time it's completely okay if you don't do anything. Chill. There's many other things that you love. Do what you love and and some of them are having so much fun being at home with their families I know some are doing like fashion things and are doing a lot of…drawing and sketching and painting and so…you know it's uh…if you can find it, there's nothing wrong with just being still as well. Which maybe the really big lesson for this whole thing right, is…I think we got a lot of messages at the beginning where it's like, do something with this time! Which probably contributed to everyone's anxiousness, collective anxiousness where I'm like oh I'm not getting enough done! But…do you have to? It's important to just slow down and recharge and…so…
Rebekka: I especially love hearing that from folks who do dance and movement, to be still. I think that's actually very beautiful. To grant permission to do that…as a mover and shaker, you know?
Josh: Absolutely. That and when I make dances I think about contrast, and contrasting movement, and contrasting speeds, and textures, and things like that and I think in my life that's also been important so when I'm doing my intense dancing, I'm dancing all the time but I also need that time to not do that at all. And that's what feeds that other one, that's what makes the dancing so beautiful, you know? And feel so great because I am taking time and I'm sure any dancer would say this where they do take time where they're like, I don't even want to listen to music you know? Maybe not that, but maybe I don't want to listen to the music that I'm dancing to, or choreographing to..and it's just like, I just…I just need to chill out and watch some movies, play some games, snuggle some cats…
Rebekka: Snuggle the cats!
Josh: Yeah that's a…that's a go to!
Rebekka: My parting question for you is…why the kitchen?
Josh: Why the kitchen…
Rebekka: I notice that you dance in the kitchen, why the kitchen?
Josh: Ohhh what a lovely question! Thank you for that, okay! Why the kitchen? I love the kitchen. I love the kitchen. I think there's like, there's practical reasons and then there's like the emotional reasons. The practical reason is that, in my house, that is the most open space where that, from an angle, you can see. You can see my feet, my whole body. That's one. Two, if I do it in the kitchen, I have to keep the kitchen clean.
Josh: So, which means that you know, dishes, and it's funny cause like our dishwasher broke too and we're like oh my gosh! Which means you know, doing dishes and making sure it's clean so I could dance in it.
Rebekka: That's brilliant.
Josh: So that's always good because, you know, to have at least one room that looks sparkly all the time is great…when you're living in your house all the time. But the other side is I love the kitchen. I love to cook. I love to eat. I love to bake, well specifically cheesecakes. Not cookies, not other baking things…cheesecakes! I bake cheesecakes that's like my thing, I've been doing it for years.
Rebekka: That's so specific and so fantastic.
Josh: Oh my gosh I just love it! I love it. It's like a thing like even at the beginning of this I made some cheesecakes, me and my wife we made some cheesecakes, and I like delivered them to friends just to be like…hey. So we made some cheesecakes and handed them out.
Rebekka: Oh I love that.
Josh: And eventually, so we're doing an online battle for our studio, for the kids, where that they submit it and that's one of the prizes that they get a full cheesecake so…because they've heard rumours of it.
Rebekka: Well now the whole internet will know so…are you prepared?
Josh: I'm prepared. They're pretty good! I dunno, maybe it could be like my side hustle, who knows?
Rebekka: Is there anything else you'd want to add that you didn't? I always like to ask because…perhaps there's something on your mind.
Josh: You know what, I did have a thought that what is kinda neat about this is seeing, I think, people in their own habitat. For lack of a better way to say it. And I think there's something kinda connecting about that because we all see each other at these places of work, or business, or social, you know, and the odd time you have somebody come to your home and so on. But with this I've had many people in my kitchen, you know? And in my house and with the different people that I've taught, you know, you see their animals walk by and pets and a sister or a brother like come up and start dancing in front of the screen and there's…although we're lacking community we're lacking the connection…because of that, their almost…there's like a new connection that's being? And maybe even a fuller picture of who you are learning from or working with. And… there's something kinda beautiful in that vulnerability…
Rebekka: Something very human about it.
Josh: Yeah! There's something and I can't place it, I have a hard time articulating exactly what it is but there's something about it that's really really neat that, you know, that you see this different side of people. In the studio my wife is there, she pops in a lot, and she does a class or two, and all of my students know her. But like some classes know her better, some of my competitive team cause they're there a bunch of times a week, know her better. Whereas […] now, every now and then she might even walk around with like one of these koala heads or something, just to mess with the kids. Cause I'm in the kitchen too right? So she gets a drink and heads out. And then my cats have been a…specifically the one cat he's popped into a few videos and to the point where, you know, some of the younger kids they're like, where's Grayson today??
Rebekka: So charming!
Josh: Yeah there's something really neat about that. Yeah, I just wanted to share that.
Rebekka: I love that. I really do. Yeah, I think we put on this like…there's this performativity when we move through the world. Where we're, you know, very pleasant or…well, hopefully we're pleasant anyway but, I think when you see someone in their own home it's just very real, very human.
Josh: Yeah and there's something really neat about that. Something that connects in a different way.
Beyond Covid-19
Defining Movement Dance
Rebekka Gondosch
Rebekka Gondosch is an actor and arts educator based in Hamilton. She is a graduate of Trinity College Dublin's M.Phil. in Theatre and Performance program, has a B.A. in Dramatic Arts and English Language and Literature from Brock University, and a B.Ed. from Redeemer University. She was a member of Hamilton Fringe's ALERT team from 2018-2019 which co-produces Hamilton's site specific winter performance festival Frost Bites.
Release: Aeris Körper Presents Online, Interactive Residency for Arts Week
Tonight: New Vision Church Launches Do Well Concert Series Featuring A Tribe Called Red's DJ Shub
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More than 2/3 of the funding allocated in the operating stream of the City's Enrichment Funding goes to just four organizations, leaving many others underfunded.
#hamont #hamarts #hamontarts #hamontartists #hamontmusic #HamOntTheatre #dancehamont #hamontfilm #artsfunding #municipalfunding #artsinfrastructure ...


Jeremy Clarkson, Richard Hammond, and James May are well-known for their love for fast cars of all kinds – be it supercars, sports cars, or just affordable hot hatches. The latter category is being celebrated in the latest short video from The Grand Tour team on YouTube.
That's no ordinary celebration clip though. Hammond takes one of our favorite small hot hatches, the Ford Fiesta ST, and performs three crazy stunts with the only mission of breaking the internet. No, we are not kidding – the maneuvers you are about to witness in the video above are rad.
"In an attempt to appeal to the youths, Hammond tasks men to trust his driving as they backflip over, walk a tightrope, and sail away from his hot hatch," the description of the video says.
The first stunt from the clip involves the aforementioned Fiesta ST (just for the record, it's the latest generation of the model) and an athlete who has to jump over the car while it's in motion. "Right, now there is a man, I don't know his name. But it doesn't matter because in a moment I'm going to run over him," Hammond explains the basic idea. Thankfully, not everything goes according to his plan.
For the second experiment, Hammond uses "science and math" to calculate the exact speed to push another Fiesta with a small boat mounted on the roof (?!) into a lake so that the boat can sail away with a passenger onboard. Yes, it's that weird but in the end, it works out fine and no one is hurt.
The last stunt… well, we won't spoil it as it's really weird and dangerous, but fun to watch. Enjoy!


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redpajama_set_name: RedPajamaGithub


The Greenhouse Florist & Nursery, Inc. is a full service florist and nursery established in 1954. We are located at the North end of Oak Harbor, WA on beautiful Whidbey Island. The Greenhouse is a family-owned and operated business. We grow trees, fruit trees, carnivorous plants, flowers baskets and more.


text:
Christopher or Chris Buckley may refer to:

 Christopher Buckley (novelist) (born 1952), American political satirist
 Christopher Buckley (poet) (born 1948), American poet
 Christopher Buckley (journalist) (1905–1950), British journalist and historian
 Chris Buckley (footballer) (1886–1973), English football player
 Christopher Augustine Buckley (1845–1922), American political boss

redpajama_set_name: RedPajamaWikipedia


South African territory: Solidarity statement to comrades in Brazil by Abahlali baseMjondolo after the fascist Bolsonaro came to power in Brazil.
For a number of years our movement has enjoyed close relationships with various movements in the left in South America. This has included the Movimento dos Trabalhadores Sem Terra (MST), known in English as the Landless Workers' Movement, in Brazil. Many of our comrades have spent a lot of time with the MST in Brazil.
We have also been pleased to build a relationship with Movimento dos Trabalhadores Sem Teto (MTST), known in English as the Homeless Workers Movement, also from Brazil. This year we had the honour of hosting comrades from the MTST in Durban.
The recent elections in Brazil have been won by the extreme right. This is a disaster for democracy. Jair Bolsonaro, who will be the new president, has described organisations like the MST and the MTST as 'terrorists' and land occupations and road blockades as 'terrorist activities'. It is clear that the right will militarise the state and attack the popular movements of the left, and rule the poor with even more violence. Poor people in general, and black and gay people in particular, are at serious risk.
There have already been attacks on progressive media, progressive spaces in the universities and black and gay people. Our comrades in Brazil fear that a serious attack on the left, and in particular the popular movements like the MST and MTST, is a real and urgent danger.
We condemn the raids that have already been carried out against progressive forces in the media and the universities and express our full support for MST, MTST and all other forces of the left in Brazil that must now confront the reality that serious repression is inevitable.
We commit ourselves to standing firm in solidarity with our comrades in Brazil and call on all our comrades in South Africa, and around the world to do the same, especially organised membership based formations like popular movements and trade unions. We are encouraged to see how many of our comrades around the world are watching the situation in Brazil and are willing to act in whatever way they can to be in solidarity with the movements and people of Brazil.
Abahlali baseMjondolo, October 31, 2018.


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Il Bank Austria Tennis Trophy 1992 è stato un torneo di tennis giocato sintetico indoor del Wiener Stadthalle di Vienna in Austria. È stata la 18ª edizione del torneo che fa parte della categoria ATP World Series nell'ambito dell'ATP Tour 1992. Il torneo si è giocato dal 19 al 26 ottobre 1992.

Campioni

Singolare maschile

 Petr Korda ha battuto in finale  Gianluca Pozzi 6–3, 6–2, 5–7, 6–1

Doppio maschile

 Ronnie Båthman /  Anders Järryd hanno battuto in finale  Kent Kinnear /  Udo Riglewski 6–3, 7–5

Collegamenti esterni

ATP Tour 1992


This year, event was attended by 456 delegates and 77 speakers from Russia, USA, Canada, China, Japan, Austria, Finland, Sweden, and Estonia. 30 regions of Russia were represented among the Forum's participants. As always, the event's target audiences included industry experts, entrepreneurs, politicians, researchers, and forestry professionals. The Forum's information support was provided by over 35 industry-specific and business media outlets.
Among the participants of the St. Petersburg Forestry Forum were: Kohlbach Energieanlagen GmbH; Springer Maschinenfabrik GmbH; Russian Timber Group; SC «Company group «Vologodskiye lesopromyshlenniki»; HQ SVEZA; PDK "Apsheronsk"; Rusforest; Novoyeniseiskiy Wood Chemical Complex" (ZAO); Inzenskiy DOZ; Hasslaherles; Mondi SLPK; RFP Group; BNBMG Group Forest Products;Metsa Group; Mayr-Melnhof Holz; Stora Enso; International Paper; IKEA Industry Tikhvin LLC; Arkhangelsk Pulp and Paper Mill and many others.
Igor Kirsanov, CEO of the RESTEC® Exhibition Company, said in his welcoming speech to participants.
Overall, the Forum's two-day program included 4 round tables and 3 themed conferences, which allowed the participants to discuss a broad range of topics in addition to the ones mentioned above: wooden housing construction as a driver of the Russia's forestry industrial complex; the role of Russian manufacturers in the global production of birch plywood; legislation on sawn timber; new forestry methods; and finally, the use of bioenergy and biotechnology in the forestry complex.
According to delegates' and speakers' reviews, the Forum has, once again, reaffirmed its reputation as one of the Russian forestry's most efficient business platforms. Most of the participants are already making plans to attend the next year's forum.


Have you ever bumped into the same topic over and over again? I keep on running into the topic of Biblical translation. I read How the Bible Works; An Anthropological Study of Evangelical Biblicism by Brian Malley with one book group. And I am reading Eat This Book by Eugene Peterson with another group. Then last Friday,I read my friend's blog about versions of the Bible.
This may mean nothing more than I need to expand the kind of books and blogs I read. ( So today at the library I checked out four novels and Team of Rivals). Nevertheless, I have spent some time thinking about why we Christians have so many translations of the Bible and what that might mean.
The multiplicity of translations is a relatively recent event. As you will recall, one of the reformers' daring ideas was that people should be able to read Scripture in their own languages. And the translating has been nonstop ever since.
I want to consider two aspects of translation today. The first is our habit of translating the Bible into a variety of different languages. There are groups dedicated to translating the Bible into every language. The Wycliffe Bible Translators may be one of the best known groups. Why Christians do this is, I think, fairly simple. We are called to spread the Good News. Jesus tells the disciples to go out into the world- to the ends of the earth in Matthew 28 . And in Acts 2 each person hears the gospel in their own language rather than miraculously being able to understand Greek (or whatever language the disciples were speaking). It seems a logical step, once there are Christian writings, to translate them into other languages.
The second aspect of translation concerns the multitude of English language translations. My friend suggests in his blog that this has more to do with the variety of theological viewpoints held by the groups doing the translation than significant translation issues. I suspect he is right. Translation always involves interpretation. Words can have more than one meaning and knowing which one was originally intended can be open to interpretation.
But there is, as always, a theological concern here as well. Christians believe the Bible is the word of God. Having a variety of translations that are not exactly the same seems to suggest a certain fluidity about what the word of God actually is. How can several versions of the Bible each be the word of God?
Some folks might answer that question by saying that they can't. We must have one version that is The Bible and the remaining texts are close but in the end not adequate. Or one could say that the differences between the various texts are minor and don't affect the overall message of the Bible.
But those answers beg the question. What is the word of God and how do we recognize it? It seems to me, when we say the Bible is the word of God we are not saying the Bible is the words of God. Inspired text is not dictated text. In fact we don't have the original copies of any of the books in the Bible. So there is necessarily a certain level of trust involved.
We need to be able to trust the translators, but that's not what I'm talking about.
The one whom we trust is God. We trust that God through the Holy Spirit is present and active in the reading and the translating and the living. We trust that even though fallible humans are involved in the writing and translating and interpretation of the text, the Spirit is present in that process.
This doesn't mean that anything goes- that any attempt at translation, any interpretation is "fixed" somehow by the Holy Spirit. We need to be careful and thoughtful. And we need to take proper advantage of the various translations.
The word of God to us is sometimes simple but often complex. Sometimes the varieties of translations can help us comprehend the subtleties of the original language. We can glimpse a richer, more complex interpretation. God's word comes to us through words. Words require interpretation by humans. And the Word requires interpretation by a person.
Perhaps that's why my tradition talks about the Bible as the written word which points to the living Word, Jesus Christ. The Word of God is not a book, it's a person.
If you are interested in the closely related topic of authority and Biblical authority, I would recommend N.T. Wright's book The Last Word. You can get a taste of his ideas from this article, "How Can the Bible Be Authoritiative" found at the N.T. Wright page.
Posted in Bible, Christianity. Tagged Bible, Biblical interpretation, Biblical translation, Bill Tammeus, Brian Malley, Eat This Book, Eugene Peterson, How the Bible Works, N.T.Wright, The Last Word.
This is the kind of stuff that rattles around in my mind. I think you're on the right track with focusing on the Word of God rather than the words of God–and trusting God to make the Word alive. Jesus is the Word–the expression of God that communicates to us. It's his story and life that gives life to everything.


The latest air particulate air sample data is posted (table 2) for the remaining routine CEMP stations for the time period 3/13-3/30/2011.
The air sampling results table has been reorganized into two separate tables to allow easier identification of trends.
On March 11, 2011, a large earthquake and resulting tsunami damaged the Fukushima Nuclear Power Plant in Japan. The damage caused the failure of cooling and safety systems resulting in the atmospheric release of radiological materials from the reactor site. In response, the CEMP installed additional air samplers at existing sampling stations in our network to determine if radiological materials could be detected from the incident.
On March 21, air samplers equipped with glass fiber filters backed by charcoal cartridges were co-located with existing CEMP routine air samplers at the Las Vegas and Henderson stations. These samplers have the capabilities of collecting air particulates as well as iodine not attached to dust particles. Samples were collected every two to three days through April 4 and sent to UNLV-RSL for gamma spectroscopy analysis. In addition, particulate air-sample filters were collected from the routine CEMP samplers located in Las Vegas, Henderson, and Boulder City. These samples are normally collected every two weeks but were pulled early to coincide with the first set of samples from the charcoal-filter equipped units. The routine air filters from the remaining CEMP stations will also be sent for gamma-spectroscopy analysis as they are received under the routine collection schedule.
The radioactive isotopes iodine-131, cesium-134 and 137, xenon-133, and tellurium-132 were initially detected in air samples collected at the CEMP air-monitoring stations in Las Vegas and Henderson, NV, during the week of March 20, 2011. The detection of these isotopes is consistent with the release and subsequent atmospheric transport of volatile radioactive isotopes from the nuclear power plant accident that occurred in Fukushima, Japan, on March 11, 2011.
From a public health standpoint, it is the measurements of the isotopes of iodine 131 and cesium-137 that are of most interest. The reason for this interest is because if high concentrations of iodine-131 are inhaled or ingested, the radioactive iodine can concentrate in the thyroid and thereby increase the risk for cancer in that organ. Additionally, cesium is chemically similar to potassium and so will behave like potassium in the body, therefore inhalation or ingestion of high concentrations of radioactive cesium can build up in multiple locations throughout the body, which can lead to an increase in risk for various cancers.
The highest concentrations of iodine-131 and cesium-137 detected by the CEMP air-monitoring stations in Las Vegas and Henderson, NV, likely peaked in the sampling period between March 23 and March 25, and have been decreasing significantly since then. Furthermore, radioactive iodine-131 dissipates (by radioactive decay) quickly, falling by half every eight days, so if no more is produced, it is essentially gone in 80 days. Even though radioactive cesium-137 has a half life (30 years) that is much longer than that of iodine-131 (only 8 days), experts who studied exposure to radioactive emissions from the Chernobyl Nuclear Power Plant accident could not link an increase in cancers to short-term exposures to such low concentrations of radioactivity from iodine-131 and cesium-137 as are being measured from Japan at the CEMP air-monitoring stations to date. Also, these small activity concentrations of iodine-131 and cesium-137 have been detected by the CEMP air-monitoring stations over a short-time period, therefore exposures also will be of short duration. Consequently, the small activity concentrations of iodine-131 and cesium-137 detected by the CEMP air-monitoring stations from the Fukushima NPP accident in Japan, in combination with the short duration of exposure expected means that there is no public health hazard at this time. Substantiating this point is the fact that even an intake over a 16-day period of the highest concentrations measured at the CEMP air-monitoring stations (between March 23 and March 25) would yield essentially the same additional dose as that from exposure to cosmic rays during a round trip airplane flight between New York and Los Angeles (3 milli-rem or 30 micro-Sv).
Henderson, NV 3/21 - 3/23/2011 N.D. 4.3E-4 1.8E-5 N.D. N.D.
Henderson, NV 3/25 - 3/28/2011 6.1E-6 2.4E-4 N.D. N.D. N.D.
Henderson, NV 3/28 - 3/30/2011 N.D. 1.8E-4 N.D. N.D. N.D.
Henderson, NV 3/30 - 4/1/2011 N.D. 2.6E-5 N.D. N.D. N.D.
Henderson, NV 4/1 - 4/4/2011 N.D. 3.13E-5 N.D. N.D. N.D.
Las Vegas, NV 3/21 - 3/23/2011 N.D. 5.0E-4 2.4E-5 N.D. N.D.
Las Vegas, NV 3/28 - 3/30/2011 N.D. 1.6E-4 N.D. N.D. N.D.
Las Vegas, NV 3/30 - 4/1/2011 N.D. 4.8E-5 N.D. N.D. N.D.
Las Vegas, NV 4/1 - 4/4/2011 N.D. 3.43E-5 N.D. N.D. N.D.
The data shown in Table 2 represent two main subgroups of analyses. The samples collected from the first eight sampling locations (Boulder City through St. George) were analyzed within days after collection. Isotopes of Cs-137, Cs-134, I-131 and Te-132 were detected in this sample group as a result to the immediate response by CEMP to determine whether measureable radioactivity emitted from the damaged nuclear power plants near Fukushima Japan could be detected in Nevada. The remaining samples for the CEMP network were collected and analyzed under the routine collection procedures and schedule in place for the CEMP. As can be observed in Table 2, the samples from this group of locations (Overton through Tecopa) show only the detection of Cs-137 and Cs-134. I-131 and Te-132 are notably absent. These two isotopes have a very short half-life, I-131 (8 days) and Te-132 (3.2 days), relative to the Cs isotopes. Because there is a one month lag time between collection and analysis for routine CEMP samples, and only trace amounts of activity from Japan were being collected, I-131 and Te-132 in these samples had decayed to non-detectable levels.
1 The collection of these air-particulate (paper) filters from air samplers at these locations was performed earlier than scheduled to coincide with the timing of the first set of samples obtained from paper-filter and charcoal-filter equipped air sampling units.
2 Additional air-particulate samples chosen for immediate analysis to initially represent the CEMP network.


CC&G calculates, on a monthly basis, the figures required to calculate Basel III capital requirements for default fund exposures to CCPs.
Basel III parameters are available to CC&G's direct Clearing Members through the ICWS platform.
CC&G Client Services will help on any issues with credentials and retrieving reports.


text:
moshville.co.uk
Brian Fallon unveils new track "Smoke" from forthcoming debut album
The Gaslight Anthem's Brian Fallon releases his hugely anticipated debut solo album Painkillers on March 11, 2016 on Virgin EMI Records. The album is available for fans to pre-order, with newly unveiled song "Smoke" available as an instant download. Also available to download and stream is the lead single from the album, "A Wonderful Life". Fallon […]

redpajama_set_name: RedPajamaCommonCrawl


text:
The Inter-American Institute for Cooperation on Agriculture (IICA) is the specialized agency for agriculture of the Inter-American System that supports the efforts of Member States to achieve agricultural development and rural well-being.
The Institute provides cooperation services through close and permanent work with its 34 Member States, addressing their needs in a timely manner. Without a doubt, IICA's most valuable asset is the close relationship it maintains with the beneficiaries of its work. We have broad experience in areas such as technology and innovation for agriculture, agricultural health, food safety and quality, international agricultural trade, family farming, rural development, natural resource management and the bioeconomy.
Our mission is to encourage, promote and support Member States in their efforts to achieve agricultural development and rural well-being through international technical cooperation of excellence.
Our vision is to be a modern and efficient institution supported by a platform of human resources and processes that are capable of mobilizing the knowledge available in the region and around the world, with the aim of achieving a competitive, inclusive and sustainable agriculture sector that takes advantage of opportunities to contribute to economic growth and development as well as to foster greater rural well-being and sustainable management of its natural capital.
The Inter-American Institute of Agricultural Sciences (IICA) was founded, and its headquarters were established in Turrialba, Costa Rica.
Following the creation of the OAS, IICA became the specialized agency for agriculture of the Inter-American System.
The new Headquarters was officially opened in San Isidro de Coronado.
The Inter-American Board of Agriculture (IABA) was created as the highest governing body. The organization was also renamed as the Inter-American Institute for Cooperation on Agriculture. By that time, membership had climbed to 29 countries.
Argentinean Manuel Otero began his administration (period 2018-2022), and the 2018-2022 Medium-term Plan (MTP) came into operation.
MEMBERS STATES
Republic of Turkey
ASSOCIATE COUNTRIE


This year's Santa Paws will be at One Step Beyond's newly opened office in San Carlos. There are lots of parking spot behind the building and a lot bigger space. Please come in from the front door.
Bring your pets and kids for a photo with Santa!


text:
using System;
using LanguageExt.ClassInstances;
using Xunit;
using static LanguageExt.Prelude;

namespace LanguageExt.Tests.Transformer.Traverse.TryOptionT.Collections
{
    public class LstTryOption
    {
        [Fact]
        public void EmptyLstIsSuccEmptyLst()
        {
            Lst<TryOption<int>> ma = Empty;

            var mb = ma.Sequence();

            var mc = TryOptionSucc(Lst<int>.Empty);

            Assert.True(default(EqTryOption<Lst<int>>).Equals(mb, mc));
        }

        [Fact]
        public void LstSuccsIsSuccLsts()
        {
            var ma = List(TryOptionSucc(1), TryOptionSucc(2), TryOptionSucc(3));

            var mb = ma.Sequence();

            var mc = TryOptionSucc(List(1, 2, 3));

            Assert.True(default(EqTryOption<Lst<int>>).Equals(mb, mc));
        }

        [Fact]
        public void LstSuccAndFailIsFail()
        {
            var ma = List(TryOptionSucc(1), TryOptionSucc(2), TryOptionFail<int>(new Exception("fail")));

            var mb = ma.Sequence();

            var mc = TryOptionFail<Lst<int>>(new Exception("fail"));

            Assert.True(default(EqTryOption<Lst<int>>).Equals(mb, mc));
        }
    }
}


At a press event in Stockholm, Sweden today, Skype confirmed it is evaluating the addition of a typing suppression feature to its desktop clients that will automatically filter the sound of your fingers hitting the keys. Unfortunately, the Microsoft-owned company isn't ready to ship the functionality yet, despite it being available in its enterprise-focused Lync tool.
David Hands, Program Manager of Skype's Audio and Video Processing team, discussed the feature in depth and showed a demo of Lync's implementation, which frankly works extremely well. The suppression works automatically: it doesn't have to be turned on, which makes it particularly useful in conference calls.
Hands did tell TNW, however, that the company does see value in typing suppression on Skype as well. When asked about when Skype clients would get the feature, however, he could not give a specific timeframe.
While Hands noted Microsoft believes the feature is much more useful on the enterprise side, he was very clear that there is interest from the company on the consumer side as well. As someone who hasn't used Lync since working in an office, I can definitely agree: Skype is being used increasingly more in business calls, and this is the type of feature that many would love to see.
It's worth noting that Google+ Hangouts added a similar feature back in April. While Google's implementation is much more rudimentary (it merely mutes your microphone when you start typing, as opposed to actually filtering out the typing noise), the job still gets done.
Hands noted that there is a lot more work to be done as the company's enterprise and consumer tools continue to overlap. This is of course part of Microsoft's broader strategy of porting functionality to and from both Skype and Lync.
Disclosure: Microsoft paid for The Next Web's trip to Skype's Stockholm offices but has no influence at all over anything we publish.


The spotlight is the big dog of our camping light collection. These powerful devices are capable of illuminating huge swaths of land, and are ideal for night navigation. Our spotlight collection offers a variety of heavy duty models with up to 40 hours of run time. We carry both handheld and swivel spotlight models to meet your needs, in addition to spotlight products specially-designed for illuminating water. We also carry strobe lamps, which can be seen for up to 3 miles in clear conditions.
Want to learn more about our spotlight collection? Call or email our friendly customer service staff and they'll be happy to help you find the right fit for your needs.
My dad when I was small always had this kind of light and it seems these lights now are not as bright and as good as it was then but I still like the light.
I wanted power and I got it with this searchlight. The light easily cuts through the darkness of our ranch. But buyer should pay attention to its size and weight. It's bulky and heavy but it sure does work.
For the price it's a good spotlight! It looks and feels like its made with cheap parts but it serve its purpose and lights up every time.
What a spotlight! A little heavier than I expected, but it has the brightest light. I am very satisfied!
The flashlight is super bright, the auxiliary LED light lights it up great, the weather radio is superb, am/fm radio has excellent reception range, fast charging, and holds a long battery. For the price, this is the BEST flashlight on the market!!
It does a good job!


Furniture made during this arts and crafts movement did not reflect a single style, but rather a theory of design that reunited the hand and eye of the maker. In Massachusetts, a state with a strong interest in history, objects made in the colonial revival style were a significant contribution to the arts and crafts movement. By about 1920, the extraordinary entrepreneur Wallace Nutting popularized the "early American" aesthetic, which remains a significant part of the furniture market to this day.
Following the lead of English authors and theorists such as John Ruskin and William Morris, practitioners of the arts and crafts reform movement in America sought a return to the ideal conditions of pre-industrial life. They sought to reunite the designer and craftsman, and took joy in the creation of "honest," simple objects, rejecting what was seen as the overblown, over-ornamented travesty of factory-produced objects.
The Society of Arts and Crafts, Boston, was incorporated in 1897 in order to "bring Designers and Workmen into mutually helpful relations, and to encourage workmen to execute designs of their own." The Society strove to foster in craftsmen "an appreciation of the dignity and the value of good design" and to counteract what was seen as "the desire for over ornamentation and specious originality." In terms that plainly reveal the drive for new simplicity, the Society determined to "insist upon the necessity of sobriety and restraint, of ordered arrangement, of due regard for the relation between the form of its object and its use, and of harmony and fitness in the decorations put upon it." A similar group was soon started in Deerfield as the tenets of the movement gained momentum.
One leader of the new movement was Francis H. Bacon, who designed furniture for A. H. Davenport and Company. His pieces were often used in architectural commissions by the firm of the famous architect Henry Hobson Richardson. As the arts and crafts movement took hold, other Massachusetts craftsmen and designers followed Bacon's lead, often producing objects that were redolent of the colonial era that was so beloved by the state.
Bakker, Keith. "H.H. Richardson's Furnishings." In The Makers of Trinity Church in the City of Boston, ed. James F. O'Gorman, 83-103. Amherst: University of Massachusetts Press in association with Trinity Church in the City of Boston, 2004.
Cooke, Edward S., Jr. ""The Aesthetics of Craftsmanship and the Presence of the Past": Boston Furniture-Making and Wood-Carving." In Inspiring Reform: Boston's Arts and Crafts Movement, ed. Merilee Boyd Meyer, 58-69. Wellesley, Mass.: Davis Museum and Cultural Center, 1997.
Farnam, Anne. "A.H. Davenport and Company, Boston Furniture Makers." Antiques 109, no. 5 (May 1976): 1048-55.
Farnam, Anne. "H.H. Richardson and A.H. Davenport: Architecture and Furniture as Big Business in America's Gilded Age." In Tools and Technologies: America's Wooden Age, ed. Paul B. Kebabian and William C. Lipke, 80-92. Burlington, Vt.: Robert Hull Fleming Museu, University of Vermont, 1979.
Kaplan, Wendy, et al. "The Art That is Life": The Arts and Crafts Movement in America, 1875-1920. Boston: Little, Brown for the Museum of Fine Arts, Boston, a New York Graphic Society Book, 1987.
Prouty, F. Shirley. Master Carver from Germany's Passion Play Village to America's Finest Sanctuaries: Johannes Kirchmayer, 1860-1930. Foreword by Gerald W.R. Ward. Portsmouth, N.H.: Peter E. Randall, 2007.
Armchair for the Woburn Public Library. Probably designed by H.H. Richardson; possibly manufactured by A. H. Davenport & Company. Boston, MA, ca. 1878. Oak, leather. Collection of Museum of Fine Arts, Boston.
One of America's most influential architects of the nineteenth century, Henry Hobson Richardson is best known for his original interpretation of early medieval building styles in modern architecture; he himself described the style as "a free rendering of the French Romanesque." As an important figure in the design-reform movement of the period, he designed furnishings and interiors integrated with the overall architectural scheme of his libraries, churches, and other public buildings. For the Woburn Public Library (sometimes called Winn Memorial Library) in Woburn, Massachusetts — the first of several public library commissions, constructed from 1876 to 1879 — Richardson designed this chair to harmonize with the curved lines of the wooden barrel-vaulted ceiling in the book room and the picturesque, neo-medieval style of the building. The chair reveals the influence of British architects and design reformers, including Augustus Welby Northmore Pugin, Bruce Talbert, William Morris, and others who advocated a return to the "honest" design principles of medieval furniture. Richardson intended its solid oak frame with chamfered, or angled, edges and deliberately exposed joinery to suggest the sturdy character of medieval furniture so admired by the English reformers. The chair's curving, crossed members and pared-down structure may be indebted to Gothic-inspired designs by Pugin and Talbert, including X-frame chairs and tables. Nevertheless, Richardson's chair was an original form, which despite its massive scale is visually lightened by its spare carved ornament and its unusual cantilevered arms.
Small joined bed with high, cantilevered headboard; frame-and-panel backboard decorated with a central angel; sides of headboard with diamond-piercing in lower section containing carved and gilt flower, and with carved and gilt decoration at skirt, and with engaged quarter-columns at rear with carved and gilt rosettes; upper portion of side panels contain freestanding gilt and polychrome carved angels, flanked by oval cut-outs, supporting projecting roof; roof of board and batten construction, with carved gilt inscription against blue ground on horizontal strips; low shaped sides tenoned and bolted to head- and footboards (replacing original higher sides with vertical slats); footboard with three panels and with inward facing angels and other decoration echoing headboard.
Ornately carved bookcase from the Joy Street home of Robert Treat Paine; center doors engraved with motto "Wisdom is better than rubies." Design attributed to architect H.H. Richardson in the 1911 estate inventory with the addition of "Norcross 800." presumed to be the maker and original price. Given to the Society by Kate L. Paine, of Bermuda, in 1972.
This settle represents the collaboration between architect and furniture manufacturer that typifies high quality Boston-made furniture of the late nineteenth and early twentieth centuries. It was made under the direction of architect Charles Donagh Maginnis (1867-1955) by Irving and Casson—A. H. Davenport for the front hall of the architect's Brookline Home. Maginnis specialized in buildings built in the Gothic style. Irving and Casson—A. H. Davenport began as separate firms with workshops in East Cambridge, Massachusetts in the 1880s and formally merged in 1914.


The Samsung Galaxy Tab E is a useful device driven by a robust 1.3 GHz processor and running on Android platform. The Tablet is equipped with 8 GB memory storage. It also features a convenient 9.6-inch display that provides clear visuals. This Tablet supports Wi-Fi connectivity and lets its users wirelessly surf the Web, check e-mails, or stream videos. The product is available in Black. Its weight is 1.08 lbs.
The Samsung Galaxy Tab S2 Tablet is driven by a robust octa-core processor and runs on the Android OS. This tablet is equipped with a 32 GB memory that lets you store multimedia files or documents. Its 8-inch display with a resolution of 2048x1536 pixels provides clear visuals. With its Wi-Fi and Bluetooth connectivity, this Samsung tablet lets you surf the Internet, check emails or stream videos on the go. In addition, it features a built-in 8 MP camera that lets you capture vivid images.
The Samsung Galaxy Tab S2 features a convenient 9.7-inch display that provides clear visuals. It is powered by a 1.9 GHz processor and the Android OS. This device is equipped with 128 GB storage capacity. Furthermore, the Samsung device has a built-in 8-megapixel camera.
The Samsung Galaxy Tab S2 is a useful device driven by a robust 1.9 GHz processor and running on Android platform. The Tablet is equipped with 32 GB memory storage. It also features a convenient 9.7-inch display that provides clear visuals. This Tablet supports Wi-Fi connectivity and lets its users wirelessly surf the Web, check e-mails, or stream videos. The product is available in Gold.
Fitting comfortably in the hand, this white Samsung Galaxy Tab T280N tablet computer is 10.88 cm wide and has a 7-inch display size. With WiFi connectivity, a 1.3 GHz processor and an 8 GB hard drive, giving you plenty of capacity to surf the internet, play games, view films, listen to music, and tweet, like, share, and comment to your heart's content on social media. It is carrier unlocked so that you can choose your service provider.


text:
\section{Introduction} \label{sec:intro}

If the dark matter-nucleon scattering matrix element is spin-dependent, then one of the leading
detection strategies is to search for the neutrinos that arise from the annihilation
of dark matter that has collected in the Sun~\cite{Silk:1985ax, Press:1985ug, Krauss:1985ks}.  Some types of neutrino detectors, such
as liquid scintillation or liquid argon detectors, can provide very good energy resolution
for an electron \mbox{(anti)neutrino.}  In this work, we describe the enhanced sensitivity of these detectors
to dark matter candidates that annihilate to monoenergetic neutrinos, and in particular
determine the current limits that can be placed by the Kamioka Liquid Scintillator Antineutrino Detector (KamLAND) with data that has already been taken.

WIMP annihilation directly to neutrino-antineutrino final states, $XX \rightarrow \nu \bar\nu$, is typically considered to be disfavored.
Indeed, if the dark matter candidate is a Majorana fermion, as is found in the MSSM for neutralino dark matter, direct annihilation to $\nu \bar\nu$ is strongly suppressed:
The initial state consists of two identical fermions, so its wavefunction must be totally antisymmetric,
implying that $s$-wave annihilation can only occur from a $J=0$ initial state.  For a $J=0$ $\nu \bar\nu$
final state, the neutrino and antineutrino must have the same helicity, so one would expect
this amplitude to be suppressed by the neutrino mass, assuming minimal flavor violation.  This
result relies on the assumption that dark matter is its own anti-particle and also on the assumption of minimal flavor violation;
if either assumption fails, the process $XX \rightarrow \nu \bar\nu$ may, in fact, have a large branching fraction.
Explicit models for which one would expect non-negligible annihilation to monoenergetic neutrino final states have been studied in~\cite{Belotsky:2001ka, Belotsky:2002sv, Barger:2007hj, Belotsky:2008vh, Esmaili:2009ks, Esmaili:2010wa}.

Searches for neutrinos from dark matter annihilation, in the Sun or elsewhere, are sensitive to the expected neutrino energy spectrum.
If dark matter annihilates primarily to heavy Standard Model particles, such as $W$-bosons, $b$-quarks,
or $\tau$-leptons, then the decay of these products produces a continuum neutrino spectrum over a range of energies, with a high energy cut-off near the mass of the dark matter particle.
In this case, experimental searches must consider possible excesses of events over the relevant, potentially very broad, range of energies.
If, on the other hand, dark matter annihilates directly to $\nu \bar{\nu}$ final states, the signal would manifest as monoenergetic neutrinos and antineutrinos.

The energy of an electron (anti)neutrino can be measured to high
precision by liquid scintillation detectors~\cite{Learned:2009rv,Peltoniemi:2009xx} and liquid argon detectors~\cite{Adams:2013qkq}.
A high energy electron neutrino produces an $e^\pm$ through a deep inelastic charged-current interaction, and the energy of the electron shower
as well as that of the scattered parton can be well-measured at those types of detectors.  The atmospheric neutrino
background to a search for monoenergetic lines is greatly reduced as the energy resolution of the detector is improved. Furthermore, if there are a sufficiently large number of background events, it may also be possible to characterize and subtract the atmospheric background using sideband techniques.  Thus
liquid scintillation or liquid argon detectors may provide impressive sensitivity to dark matter candidates that annihilate to monoenergetic neutrinos.

Previous studies of monoenergetic neutrino signals from dark matter annihilation in the Sun have focused on heavier WIMPs accessible to the IceCube neutrino detector.  By contrast, the detectors considered here are limited in their sensitivity to low WIMP masses only by the physics of WIMP interactions within the Sun itself (evaporation)~\cite{WIMPevaporation}, and not by a loss of sensitivity to the relevant range of neutrino energies.  The detectors considered here therefore represent an excellent complement to neutrino searches for heavier WIMPs with masses $\gtrsim 100$ GeV.

In section II, we describe the general analysis underlying a monoenergetic neutrino search
at a liquid scintillation-type detector.
In section III, we implement this analysis for the specific case of KamLAND.  We conclude
with a discussion of our results in section IV.

\section{Analysis}

We focus on a search for monoenergetic electron (anti)neutrinos arising from dark matter
annihilation, $XX \rightarrow \nu_l \bar\nu_l$, and assume the annihilation cross section is flavor-independent.
A deep inelastic charged-current interaction (for example, $\nu_e d \rightarrow
e^- u$) within the target will produce electromagnetic and hadronic showers, the energies of which can be measured quite well in
liquid scintillation or liquid argon detectors.  Moreover, the direction of the electromagnetic shower
can also be reconstructed\footnote{In a liquid scintillation detector, the timing of illumination of the various photomultiplier
tubes can be used to reconstruct the direction of the electron or positron track within the scintillator~\cite{Learned:2009rv,Peltoniemi:2009xx}.},
providing a good measurement of the outgoing electron or positron's direction.
The energy resolution and angular resolution possible at liquid scintillation-type neutrino detectors make these instruments extremely powerful tools with which to search for dark matter.

\subsection{Neutrino Flux from Dark Matter Annihilation}

In general, the differential flux of monoenergetic neutrinos produced by dark matter annihilation can be
expressed as
\begin{eqnarray}
{d^2\Phi_{DM} \over d\Omega dE} &=& {1 \over 4\pi} B_\nu \left[ \int dr\, {d\Gamma \over dV } \right] \delta (E_\nu - m_X) ,
\label{eq:flux}\end{eqnarray}
where $d\Gamma / dV$ is the rate of dark matter annihilation per volume,
and $B_\nu$ is the branching fraction for dark matter to annihilate to monoenergetic neutrinos, which we
take to be flavor-independent.
The differential antineutrino flux is the same.

The Sun may be an important source of monoenergetic neutrinos from dark matter annihilations.
If dark matter in the Sun is in equilibrium, then the annihilation rate is $1/2$ the rate at
which dark matter is captured via scattering against solar nuclei (see, eg.,~\cite{Peter:2009mk}).  We assume that dark matter-nucleon scattering is
a spin-dependent contact interaction, as spin-independent scattering is tightly constrained by
direct detection experiments.  We may then express this capture rate~\cite{Gould:1987ir} as
$\Gamma_C = C_0^{SD}(m_X) \times \sigma_{\rm SD}^p \times [(\rho_X / \rho_\odot) (\bar v / 270~\text{km} / \text{s})^{-1}] $,
where $\sigma_{\rm SD}^p$ is the dark matter-proton spin-dependent scattering cross section,
$\bar v$ is the dark matter velocity dispersion of a Maxwell-Boltzmann distribution, and
where values of $C_0^{SD}(m_X)$ may be found, for example, in~\cite{Gao:2011bq}.  We then find
\begin{eqnarray}
\int dr\, {d\Gamma \over dV } &=& {1 \over 2 r_\oplus^2} C_0^{SD} (m_X) \sigma_{\rm SD}^p
\left[\left( {\rho_X \over \rho_\odot} \right) \left({\bar v \over 270~\text{km} / \text{s}} \right)^{-1}  \right]
\delta (\Delta \Omega) ,
\label{eq:SunRate}
\end{eqnarray}
where $r_\oplus = 1~{\rm AU}$ is the Earth-Sun distance, and the $\delta$-function imposes the constraint that
neutrinos will arrive from the direction of the Sun.  If we take, as a benchmark, $\langle \sigma_A v \rangle =
1~\text{pb} \times c$ and $m_X = 10~\text{GeV}$, then the Sun is in equilibrium if $\sigma_{\rm SD}^p \gtrsim 3 \times 10^{-7}~\text{pb}$~\cite{Kumar:2012uh}.
Comparing the result of Eq.~\ref{eq:SunRate} (assuming $\sigma_{\rm SD}^p \gtrsim 3 \times 10^{-7}~\text{pb}$) to the integrated annihilation
rate near the Galactic Center as detailed in appendix \ref{sec:appendix}, it's clear that
the neutrino flux from the Sun is a few orders of magnitude larger than that from the
Galactic Center\footnote{For $m_X \gg 10~\text{GeV}$, the neutrino flux from the Sun and from the Galactic Center both scale as
$m_X^{-2}$, so the conclusion holds for the range of dark matter masses considered here.}.  Henceforth, we will thus focus on searches for neutrinos arising from dark matter annihilation
in the Sun\footnote{Dark matter can only be captured in the Sun if it scatters against nuclei.
However, this coupling need not imply that the dark matter annihilation branching
fraction to hadronic final states is dominant.}.

The effects of oscillations, absorption, and regeneration as neutrinos propagate in the Sun, from the Sun to the Earth, and in the Earth, have been well-studied in recent years.  Here, we consider only the energy range from 5 to 100 GeV, since evaporation from the Sun becomes significant for dark matter with $m_X\lesssim 4$ GeV~\cite{WIMPevaporation} and neutrino absorption suppressed the line signal for neutrino energies $E_{\parenbar{\nu}} \gtrsim 100$ GeV~\cite{Cirelli:2010xx}.  For the range of energies we consider, although interactions in the Sun will affect
neutrino flavor oscillations, the effect on the neutrino energy spectrum will be relatively small
(see, for example, \cite{Allahverdi:2012bi}).  For a specific detector, a more detailed analysis could
include the effect on the neutrino spectrum of matter effects in the Sun and Earth (the latter depend on the
location of the detector), but for a general analysis this will not be necessary.

Finally, for the range of WIMP masses considered here, we note that the assumption of dark matter capture-annihilation equilibrium is satisfied for total annihilation cross sections within a few orders of magnitude of the thermal benchmark, $\langle \sigma_A v \rangle = 1 \text{pb} \times c$, for spin-dependent WIMP-proton scattering cross sections of $\sigma_{SD}^p \sim 10^{-4}$ pb~\footnote{The equilibration time scales as $(\sigma_{\rm SD}^p < \sigma_A v > )^{-1/2}$.}.  The total annihilation rate in the Sun is then set by $\sigma_{SD}^p$ as in Eq.~\ref{eq:SunRate}, with a fraction $B_{\nu}$ of these annihilations resulting in monoenergetic neutrinos.
Our results are therefore sensitive to the branching fraction to monoenergetic neutrino final states, but robust with respect to the overall dark matter annihilation cross section today, which may be significantly smaller than the typically-assumed thermal scale.

\subsection{Effective Area of the Detector}

Assuming that the number of protons and neutrons in the detector target are the same,
the average neutrino-nucleon deep inelastic scattering cross sections for charged-current interactions with
$E \gg \text{GeV}$ are~\cite{Edsjo:1993pb},
\begin{eqnarray}
\sigma_{\nu N} &\sim& (6.66 \times 10^{-3} \text{pb}) \left({E \over \text{GeV}} \right) ,
\nonumber\\
\sigma_{\bar \nu N} &\sim& (3.25 \times 10^{-3} \text{pb}) \left({E \over \text{GeV}} \right) .
\end{eqnarray}
We may then express the effective area of the detector, $A_\parenbar{\nu}^{eff.}=\sigma_{\parenbar{\nu} N} \left(\frac{\rho_{det}}{m_N}\right) V$, where $\rho_{det}$ is the density of the detector material, $m_N$ is the mass of a nucleon, and $V$ is fiducial volume, for (anti)neutrino scattering as
\begin{eqnarray}
A_\nu^{eff.} &=& 2.03 \times 10^{-3} \text{cm}^2 \left({E \over \text{GeV}} \right) \left({\rho_{det} \over 1~\text{g} /\text{cm}^3 } \right)
\left({V \over 10^3~\text{m}^3 } \right),
\nonumber\\
A_{\bar \nu}^{eff.} &=& 9.88 \times 10^{-4} \text{cm}^2 \left({E \over \text{GeV}} \right)
\left({\rho_{det} \over 1~\text{g} /\text{cm}^3 } \right)
\left({V \over 10^3~\text{m}^3 }\right).
\end{eqnarray}

We will only consider events in which the $e^\pm$ falls within an angle $\theta_{cone}$ of
the Sun~\cite{Jungman:1995df}, where
\begin{eqnarray}
\theta_{cone} &=& 0.37 \sqrt{10~\text{GeV} \over E}.
\end{eqnarray}
For electron neutrinos (antineutrinos) arriving from the sun, $f_\nu$ ($f_{\bar \nu}$) is the fraction of electrons (positrons) produced
by charged-current interactions that fall within this cone.  $f_{\nu, \bar \nu}$ is roughly determined by the
angular dependence of the matrix element for left-handed quarks to scatter against left-handed neutrinos and
right-handed anti-neutrinos, respectively.  $f_{\nu, \bar \nu}$ can then be expressed as
\begin{eqnarray}
f_\nu &=& \frac{1-\beta^2}{2}\int_{\cos\theta_{cone}}^1 dx \, \frac{1}{(1-\beta x)^2}
\nonumber\\
f_{\bar{\nu}} &=& \frac{1-\beta^2}{2}\int_{\cos\theta_{cone}}^1 dx \,  \frac{1}{(1-\beta x)^2}\frac{3}{4} (1+\cos\theta_{cone})^2,
\label{eq:f_fbar}
\end{eqnarray}
where $\beta$ is the boost from center-of-mass frame to lab frame.
We find $f_\nu \approx 0.4$ and $f_{\bar \nu} \approx 0.8$, results which are mildly dependent on the (anti)neutrino energy.  In the following analysis, we use the full expression for $f_\parenbar{\nu}$ given in eq.~\ref{eq:f_fbar}.

\subsection{Signal and Background Events}

The expected number of events in a particular detector arising from dark matter annihilation can then be expressed as
\begin{eqnarray}
N^{\parenbar{\nu}_e}_{sun} &=& 0.68 \times T \left({B_\nu \over 3} \right)
\int_{E_{min}}^{E_{max}} dE \, {d\Phi_{DM} \over dE} \times A_{\parenbar{ \nu}}^{eff.} \times f_{\parenbar{ \nu}} ,
\end{eqnarray}
where $T$ is the detector runtime, $E_{min, \,max}= m_X [1 \pm (\epsilon/2)]$, and $\epsilon$ is the energy resolution of the detector.
Again, $B_\nu$ is the branching fraction for dark matter annihilation to all neutrino flavors; since we assume
that annihilation is flavor-independent, $\sim 1/3$ of the neutrinos reaching the detector will be
electron neutrinos even after including vacuum and matter oscillation effects~\cite{Lehnert:2007fv}.  The factor of $0.68$ accounts for the fact that $68\%$ of events fall within a bin of width $\epsilon$.
Similarly, the number of events due to the atmospheric neutrino background can be expressed as
\begin{eqnarray}
N^{\parenbar{\nu}_e}_{atm} &=& T \int_{E_{min}}^{E_{max}} dE \, {d^2 \Phi_{atm}^{\parenbar{\nu}_e} \over d\Omega \, dE} \times A^{eff.}_{\parenbar{\nu}}
\times \left[(2\pi)(1-\cos \theta_{cone}) \right] ,
\end{eqnarray}
where ${d^2 \Phi_{atm} \over d\Omega \, dE}$ is the atmospheric electron (anti)neutrino flux.  We use the angle averaged
atmospheric electron (anti)neutrino fluxes given in~\cite{Honda:2011nf}, which, in the relevant energy range, are well-approximated by the
power law fits
\begin{eqnarray}
{d^2 \Phi_{atm}^{\nu_e} \over d\Omega dE} &\sim&  (4.17 \times 10^{-2} \text{cm}^{-2} \text{s}^{-1} {\rm sr}^{-1} \text{GeV}^{-1} )
\times \left(0.80 + {E \over \text{GeV}} \right)^{-3.490},
\nonumber\\
{d^2 \Phi_{atm}^{\bar \nu_e} \over d\Omega dE} &\sim&  (2.42 \times 10^{-2} \text{cm}^{-2} \text{s}^{-1} {\rm sr}^{-1} \text{GeV}^{-1} )
\times \left(0.53 + {E \over \text{GeV}} \right)^{-3.417}.
\end{eqnarray}

Given the number of signal and background events expected at a neutrino detector, one can then
determine sensitivity of the detector to a dark matter model for any choices of
$m_X$ and $\sigma_{\rm SD}^p$.

\section{Bounds from KamLAND}

In this section, we apply the analysis framework above to the specific case of the KamLAND detector and the data it has accumulated over more than
10 years.
KamLAND~\cite{Eguchi:2002dm} is a liquid scintillation neutrino detector with $\rho_{det} \approx 0.8~\text{g} / \text{cm}^3$ and an approximately spherical
inner detector with volume $\sim 1000~\text{m}^3$.  We define the fiducial volume of the detector such that if a charged-current interaction produces an $e^\pm$ within the fiducial volume, at least 10 radiation lengths ($\sim 4.3~\text{m}$) will be contained within the
inner detector.  For KamLAND, the fiducial volume is $\sim 500~\text{m}^3$~\cite{Kumar:2012uh}.
If an electron (anti)neutrino with energy greater than $1~\text{GeV}$ participates
in a charged-current interaction within the fiducial volume, it is estimated that the energy of the original neutrino can be
reconstructed to within a few percent accuracy, and that approximately 3600 live-days of data are available
for such an analysis~\cite{KamLAND_energy_res}.
As a benchmark, we will take the energy resolution for this analysis to be $\epsilon =5\%$.
It is also estimated that the charged lepton flavor can be determined with very high efficiency, and that the
direction of the electromagnetic shower can be determined with a resolution much better than $\theta_{cone}$ for the
energy range of interest~\cite{Peltoniemi:2009xx}.

\begin{figure}[t]
  \centering
    \includegraphics[width=0.7\textwidth]{BGbigRLabeledPrinted.pdf}
    \caption{The expected number of background events as a function of the central bin energy for a KamLAND exposure of 3600 days with energy resolution of 1\% (solid grey), 5\% (solid black), and 10\% (dotted grey).  We also show the projected number of background events as a function of energy for a detector with an exposure 10 times larger than that of KamLAND with an energy resolution of 3\% (dashed black).  We note that the dotted grey curve also represents the expected number of background events for a detector with an exposure 10 times larger if the energy resolution is 1\%.
\label{fig:background}}
\end{figure}

We note that for the exposure of KamLAND, one expects far less than one background event within each energy
bin, whose size is determined by the energy resolution.  In Figure~\ref{fig:background}, we show the expected number of background events as a function of the central bin energy for a KamLAND exposure of 3600 days and energy resolution of 1\% (solid grey), 5\% (solid black), and 10\% (dotted grey).  We also show the projected number of background events as a function of energy for a detector with an exposure 10 times larger than that of KamLAND with an energy resolution of 3\% (dashed black).  The inset shows the low-energy regime in more detail.  It is clear that, for the exposure of KamLAND, the atmospheric neutrino background is negligible.

A 90\% confidence level upper limit on the spin-dependent dark matter-proton elastic scattering cross section as a function of dark matter mass is
obtained (see, for example, ~\cite{Feldman:1997qc}), assuming zero observed events in each relevant energy bin during 3600 KamLAND live-days.
The expected upper limit on the spin-dependent dark matter-proton scattering cross section from KamLAND is shown in Figure~\ref{fig:limitplot} as the thick black contour for $B_{\nu}=1$, $\rho_X = \rho_\odot$ and $\bar v = 270~\text{km} / \text{s}$~\footnote{As the number of signal events is proportional to $\sigma_{\rm SD}^p B_\nu (\rho_X / \rho_\odot)(\bar v / 270~\text{km} /\text{s})^{-1}$, the sensitivity for any choice of $B_\nu$, $\rho_X$ and $\bar v$ can be determined
by a simple rescaling.}, as well as the expected sensitivity of a liquid scintillation detector with a factor 10 larger exposure than KamLAND and with a $3\%$ energy resolution (thick black dashed).
 For comparison, the dashed, solid, and dotted magenta curves are the upper limits from Baikal NT200 detector~\cite{Avrorin:2014swy}, assuming dark matter annihilation to $\bar \nu_e \nu_e$, $\bar \nu_\mu \nu_\mu$ and $\bar \nu_\tau \nu_\tau$, respectively, the solid cyan curve is the upper limit from Super-Kamiokande, assuming annihilation to $\tau^+ \tau^-$~\cite{SuperKprl}, and the dashed blue contour is the upper limit from the PICO-2L Bubble Chamber dark matter experiment~\cite{PICO2Lpub}.  For clarity, we display only the leading published results (or, in the case of PICO-2L, publicly released but not yet published), omitting competitive but subleading bounds from direct and indirect searches such as PICASSO~\cite{Archambault:2012pm}, SIMPLE~\cite{Felizardo:2011uw}, COUPP~\cite{Behnke:2012ys}, the Baksan Underground Scintillator Telescope~\cite{Boliev:2013ai}, and the IceCube Neutrino Telescope~\cite{Aartsen:2012kia}.

 \begin{figure}[t]
  \centering
    \includegraphics[width=0.7\textwidth]{FClimitR3.pdf}
    \caption{90\% CL upper limit on the spin-dependent dark matter-proton elastic scattering cross section as a function of dark matter mass assuming zero events at KamLAND in 3600 days of data (thick black), as well as the expected sensitivity of a liquid scintillation detector with a factor 10 larger exposure than KamLAND and with a $3\%$ energy resolution (thick black dashed).  We assume $B_\nu =1$, $\rho_X = \rho_\odot$ and $\bar v = 270~\text{km} /\text{s}$.
    For comparison, the dashed, solid, and dotted magenta curves are the upper limits from Baikal NT200 detector~\cite{Avrorin:2014swy}, assuming dark matter annihilation to $\bar \nu_e \nu_e$, $\bar \nu_\mu \nu_\mu$ and $\bar \nu_\tau \nu_\tau$, respectively, the solid cyan curve is the upper limit from Super-Kamiokande, assuming annihilation to $\tau^+ \tau^-$~\cite{SuperKprl}, and the dashed blue contour is the upper limit from the PICO-2L Bubble Chamber dark matter experiment~\cite{PICO2Lpub}.
\label{fig:limitplot}}
\end{figure}

The estimated sensitivity is
relatively robust, even if the actual energy resolution is different from our benchmark estimate by a factor of a few.  This is clear from Fig.~\ref{fig:background} for the current KamLAND exposure of $\sim 3600$ days.  Even for an exposure 10 times larger, the atmospheric background only
approaches $\mathcal{O}(1)$ event in an energy bin for the very lowest energies considered.
For $\epsilon = 3\%$, the expected number of background events in an energy bin is never larger than 0.39, for $E_\nu = 5$ GeV, and falls to less than 0.09 for $E_\nu \geq 10$ GeV.  If a single event is observed in an energy bin, the actual sensitivity will drop by $\sim 40-50\%$.

As is clear from Figure~\ref{fig:limitplot}, at this moment, the limit obtainable from KamLAND data would be stronger than limits from traditional direct dark matter searches (i.e.~for dark matter collisions with nuclei in terrestrial detectors) for WIMP masses $\lesssim 15$ GeV, assuming dark matter annihilates to $\nu \bar{\nu}$ final states with $B_\nu=1$.  The sensitivities of neutrino telescopes such as Super-Kamiokande, Baksan, and IceCube are specific to the dark matter annihilation final state, though harder neutrino spectra generally yield stronger constraints on the scattering cross section.  For those detectors,
actual limits for monoenergetic neutrino final states are likely stronger than the limits shown here.  We encourage collaborations to perform these searches.

Finally, we note that KamLAND's sensitivity is signal-limited, due to its relatively small exposure compared to that of much larger water Cherenkov
detectors such as Super-Kamiokande.  As such, the utility of liquid scintillation detectors for searches for dark matter annihilation to
monoenergetic neutrinos can only be fully realized for detectors with a much larger exposure.  For example, for an exposure ten
times larger than our benchmark KamLAND exposure, cross sections as small as $\sigma_{SD}^p \approx 10^{-4} \,(6\times10^{-4})$ pb could be probed
for $m_X =10 \,(100)$ GeV.  Such an experiment would be an very powerful probe of the interactions of dark matter with nuclei in the Sun.  This is especially true at low WIMP masses, where liquid scintillation detectors have robust sensitivity to the WIMP-proton scattering cross section down to $m_X \approx 4$ GeV, below which evaporation from the Sun becomes significant.

\section{Conclusions}

In this work, we have considered the sensitivity of liquid scintillation neutrino
detectors to dark matter annihilation in the Sun in the case that the dark matter annihilates to
monoenergetic neutrinos.  Because liquid scintillation detectors can reconstruct with
good accuracy all of the energy of an electron (anti)neutrino interacting through a charged-current
interaction, this is essentially a search for an excess in a single energy bin.  The
resulting reduction in background greatly enhances the sensitivity of liquid scintillation
neutrino detectors.  As an example, we have considered the sensitivity that KamLAND may be
capable of, using existing data.

As may be expected, the sensitivity of liquid scintillation detectors found here exceeds those of other estimates~\cite{LS_Detector_DM_Search},
which focussed on annihilation to final states that included a continuum spectrum of neutrinos, in which case a signal would emerge over a broad range of neutrino energies rather than within a single energy bin.  With its current
exposure, KamLAND would expect far less than one background event in any single energy bin for energies $\gtrsim5$ GeV.
In fact, for any liquid scintillation detector, the expected sensitivity will increase linearly with exposure in this low-background regime
(this low-background regime should extend up to an exposure of roughly 10 times the current exposure of KamLAND for all WIMP masses considered, and to considerably larger exposure for $m_X \gtrsim 100$ GeV).  If the exposure becomes large enough that the expected number of background events in an energy bin approaches one, the assumption of zero events in any bin is, of course, no longer valid for estimating the sensitivity.

It is worth noting that liquid argon-based neutrino detectors can also reconstruct the energy and direction of
an electron shower created by a charged-current interaction.  A similar analysis could thus be performed
for such detectors.  Moreover, future liquid argon-based detectors may have a much larger exposure than KamLAND.  For
example, the LBNE far detector is foreseen to be a 34 kiloton liquid argon time projection chamber~\cite{Adams:2013qkq}.
If the energy resolution is as good as a few percent, then such detectors
could obtain competitive sensitivity, placing them among the leading experimental searches for particle dark matter.

\vskip .2in
\textbf{Acknowledgments}

We are grateful to K.~Choi, C.~Kelso, J.~G.~Learned and M.~Sakai  for useful discussions.  The work of J.~Kumar is
supported in part by NSF CAREER Grant No.~PHY-1250573. The work of P. Sandick is supported in part by NSF Grant No.~PHY-1417367.
J.~Kumar and P.~Sandick would like to thank the University of Utah and University of Hawai'i, respectively,
for their hospitality and partial support during the completion of this work.

redpajama_set_name: RedPajamaArXiv


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